1. Galactic Star Formation Science
with Integral Field Spectroscopy
Tracy Beck, STScI

2. Galactic Star Formation Science with Integral Field Spectroscopy
Introduction to the formation of sun-like stars in the Milky Way
Studies of star formation (SF) with IFUs
First uses of IFUs for SF science
Herbig Haro Objects
Young Star Binaries
Star Formation at high contrast with IFUs: A Search for IR H2 Emission from the Disks of Young Stars
Cutting Edge Science: Laser-Fed AO IFU spectroscopy of young stars
Prospects for JWST and the ELTs

3. Formation of Sun-like Stars in the Milky Way
Sub-mm continuum of protostellar cores
Shirley et al. (2000)

4. Formation of Sun-like stars in the Milky Way
Young stars with Circumstellar disks + extended Envelopes (“Class I” Protostars)
HST NICMOS Imaging of Protostars (Padgett et al. 1999)

5. Formation of Sun-like stars in the Milky Way
Young stars with Circumstellar disks, no envelope material left (“Class II” Protostars, “Classical” T Tauri Stars)
Orion Proplyds
O’Dell & Wen (1994)

6. Formation of Sun-like stars in the Milky Way
Beta Pic Debris
Disk
Dust disk dissipates in <1Gyr timescale
Meyer et al. (2008)

7. Formation of Sun-like stars in the Milky Way
“Class II” Protostars with Disks + Outflows – “Classical T Tauri Stars”

8. IFUs in Star Formation Science
MPE 3D w/ Calar Alto (3.5m)
H and K-band
Observations of T Tau
Herbst et al. “A Near-Infrared Spectral Imaging Study of T Tau” 1996 AJ v.111, 2403 8”

9. IFUs in Star Formation Science
IFUs are very powerful tools for spatially resolving emission line structures in the environments of bright T Tauri Stars
Lavalley et al. “Sub-arcsecond morphology and kinematics of the DG Tauri jet in the [O I]λ6300 line” A&A v.327, 671

10. Herbig Haro Objects HH Objects:
optical/infrared tracers of YSO jets, seen where jets from young stars plow into ambient cloud material and shock the gas into emission
Pure emission line objects
viewed in optical/infrared permitted and forbidden transitions – Ha, [O I], [N II], [S II], [FeII], trace atomic gas excited by shocks
Shock-excited H2 emission in the IR
 Natural IFU Sources
Beck et al. 2004, 2007, Lopez et al. 2008, 2010 Giannini et al. 2008
HH 46/47

11. Herbig Haro Objects HH 99B: Very sensitive VLT + SINFONI observations
Wings of the Bow Shock
Herbig Haro Objects
HH 99B:
Very sensitive VLT + SINFONI observations
170+ Emission lines detected
Many very high excitation lines of H2 and [Fe II]
Bow-shock apex shows extremely high temperature - T~6000K - revealing that the H2 molecule persists in these very high temperature regions
Giannini et al. “Near-infrared, IFU spectroscopy unravels the bow-shock HH99B“ 2008, A&A v.481, 123
H2 1-0 S(1) 2.12mm
H2 2-1S(17) 1.758mm
Head of the Bow Shock
[Fe II] mm
[Fe II] mm
HI Pab 1.28 mm
[P II] mm

12. Young Star Binaries
Most stars (50-60%) form as binary or higher order multiple systems
Understand young star binary characteristics, particularly disk and mass accretion evolution
The more massive primary star often has more active mass accretion, indicating a larger circumstellar disk reservoir of mass. I.e., preferential accretion from circumsystem material onto the more massive star in a binary
Spatially Resolved Observations of Young Star binaries 0.”1 to ~1” separations, Programs ongoing using NIFS, SINFONI & OSIRIS

13. Young Star Binaries – Z CMa
Protostellar B star (Herbig Be star) primary, FU Ori eruptive variable companion
System has become a prototype for understanding eruptive mass accretion in young star binaries
0.”1 binary observed with OASIS – 0.”11 microlenses!
OASIS observations in [OI] 6300A
Garcia et al. “Spatially resolved spectroscopy of Z Canis Majoris components” 1999, A&A v.346, 892

14. Young Star Binaries – Z CMa
The Massive Herbig Be star does drive the parsec scale outflow!
The companion is discovered for the first time to drive its own small scale jet
First detection of a collimated jet from a FU Ori outbursting variable star!
Keck OSIRIS [Fe II] 1.644mm observations of Z Cma
Whelan et al. “The 2008 Outburst of Z CMa: The First Detection of Twin Jets” 2010, ApJL v.720,L119

15. High Contrast IFU Spectroscopy in Star Formation – Gas in Circumstellar Disks
HH 30
Dust in Circumstellar Disks – Traced by infrared excess
Emission, seen in scattered light images of T Tauri stars
Gas in Circumstellar Disks – As much as 99% of the mass in circumstellar disks is in GAS not DUST
Disk Gas is traced by:
mm molecular observations of cold outer disk gas
IR emission species trace warm gas from ~terrestrial regions of disks
Most studies cannot spatially resolve the gas in the inner disk regions and measure trace components of the disks, ~70% of the disk by mass is in H2

16. The Search for IR Molecular Hydrogen Gas in Young Star Disks
FWHM ~0.”1
Gemini + NIFS IFU observations of six T Tauri Stars – all known to drive YSO outflows
K-band Continuum Images
Beck et al. “Spatially Resolved Molecular Hydrogen in the Inner 200 AU Environments of T Tauri Stars” 2008 ApJ, v.676, 472

17. The Search for IR Molecular Hydrogen Gas in Young Star Disks
From Classical T Tauri stars w/ outflows, H2 arises from shocked emission surrounding the HH flows
Herbig Haro Flows
Beck et al. “Spatially Resolved Molecular Hydrogen in the Inner 200 AU Environments of T Tauri Stars” 2008 ApJ, v.676, 472

18. IFU Observations of T Tau Across a Decade…
Herbst et al. 1996
MPE 3D Data from Calar Alto 3.5m
Jan. 1995
Beck et al. 2008
NIFS Data from Gemini-N 8m
Oct. 2005

19. The Search for Molecular Hydrogen Gas in Young Star Disks
T Tau in [Fe II]
H2 Emission
Flux
VLT + SINFONI Observations of T Tau, detection of H2 from the face-on disk around T Tau N?
Gustofsson et al. “Spatially resolved H2 emission from the disk around T Tau N” 2008
H2 Velocity
H2 Velocity
Dispersion

20. Where is the IR Molecular Hydrogen Gas in Young Star Disks?
Doing a Gemini + NIFS IFU survey of additional young stars, more than doubling the past sample – this includes stars that have evidence for dust disk gaps (from IR SED shapes), and/or “disk-like” H2 from past long-slit observations
Highlight = GG Tau A, 0.”3 binary young star, with the prototypical “Circumbinary Ring” of dust (Roddier et al. 1996) 3” *
Circumbinary Ring seen in scattered light
T. Beck, J. Bary et al. “The Search for Spatially Resolved IR H2 from the Disks of Classical T Tauri Stars” (in prep.)
Subaru CIAO Observations of GG Tau A

21. The Search for IR H2 from a Disk High Contrast for Star Formation
IR Spectrum of GG Tau A – typical of young stars
Brg
NIFS 2.12mm continuum image
of the 0.”3 GG Tau A binary
H2??
Fe I
H2!!
Looking for a signal of ~few 100 cts, on a continuum of 30K+ cts, with a photospheric Fe I feature in the way!

22. The Search for IR Molecular Hydrogen Gas in Young Star Disks
T. Beck, J. Bary et al. “The Search for Spatially Resolved IR H2 from the Disks of Classical T Tauri Stars” (in prep.)

23. The Search for IR Molecular Hydrogen Gas in Young Star Disks
H2 Emission in the Environment of GG Tau A
H2 2-1 S(1) / 1-0 S(1) line ratio not indicative of fluorescent pumping by UV photons, is consistent with X-ray heating of the gas
Gas/Dust in Protostellar binaries should NOT exist (Artymowicz & Lubow 1994):
Circumstellar: at spatial locations beyond ~1/3 of the semi-major axis of the binary (disk truncation)
Circumbinary: at spatial locations within ~3x the semi-major axis of the binary (gap clearing)
Clearing timescale ~100’s of years!
H mm
T. Beck, J. Bary et al. “The Search for Spatially Resolved IR H2 from the Disks of Classical T Tauri Stars” (in prep.)

24. The Search for IR Molecular Hydrogen Gas in Young Star Disks
40AU – Pluto’s semi-major axis
H mm
H mm
T. Beck, J. Bary et al. “The Search for Spatially Resolved IR H2 from the Disks of Classical T Tauri Stars” (in prep.)

25. Cutting Edge SF Science: Laser-Fed AO Observations of Young Stars
Pushing to Higher Mass:
Comparably few detailed spatially resolved observations of collimated outflows toward protostars with higher mass than the sun-like T Tauris.
Keck Observatory LGS AO + OSIRIS IFU Observations of the very young Herbig Ae star LkHa 233
Investigate whether the similarity on large spatial scales between outflows from T Tauri and Herbig Ae stars still holds true on finer spatial scales.
Perrin et al. “Laser Guide Star Adaptive Optics Integral Field Spectroscopy of a Tightly Collimated Bipolar Jet from the Herbig Ae star LkHa 233” 2007 ApJ, v.670, 499

26. Cutting Edge SF Science: Laser-Fed AO Observations of Young Stars
Perrin et al. “Laser Guide Star Adaptive Optics Integral Field Spectroscopy of a Tightly Collimated Bipolar Jet from the Herbig Ae star LkHa 233” 2007 ApJ, v.670, 499

27. Cutting Edge SF Science: Laser-Fed AO IFU Observations of Young Stars
Pushing to Lower Mass:
IRAS = young proto-object in the Taurus SFR (d~140pc)
Seen in the optical largely in scattered light, with a ‘bipolar’ nebula structure typical of opaque disk material along the mid-plane (Glauser et al. ’08), interpreted as a source with a disk inclined by ~63o
YOUNG! (<~1Myo!) w./ M6 type, commonly adopted SpT for young BD limit
HR Diagram fitting = substellar ~0.05Msolar (large uncertainty in models)
Andrews et al ‘08 detected the disk in sub-mm, high spatial resolution dust continuum and CO gas! extends out to >~500AU from the central source - MASSIVE disk with ~1000+ AU total extent!
Stellar mass estimate + extended massive disk! – Mdisk / Mstar ~15-20%!
HST Image From Glauser et al. 2008
Beck et al. “Laser Fed Adaptive Optics Imaging Spectroscopy of the Candidate
Proto-Brown Dwarf IRAS ” in Prep.

28. Laser-fed AO Spectral Imaging, IRAS 04158+2805
100 AU
1.644m [Fe II]
(Jet!)
2m K-band
(Scattered Light!)
2.12m H2
(Wide-Angle Outflow!)
Gemini LGS AO w/ NIFS = Goal - Determine if H2 gas traces disk material in the BD candidate environment - it doesn’t!
Data reveals fspatially resolved 2-D spectral images of a well collimated jet from a very young BD candidate
BLUE-shifted, collimated [Fe II] jet associated with the brighter lobe of the scattered light nebulosity - no redshifted jet detected
Jet Orientation consistent w/ 63o viewing disk inclination
Beck et al. “Laser Fed Adaptive Optics Imaging Spectroscopy of the Candidate
Proto-Brown Dwarf IRAS ” in Prep.

29. Laser-Fed Spectral Imaging of BD Environments
Laser-Fed AO on large ground-based telescopes is a powerful means to reveal the inner environments of BDs at high spatial resolution using IR emission lines…
Complication = BDs are optically very faint, but you need an optical tip-tilt guide star! (TTGS)
Observations of IRAS were only possible with Gemini +LGS AO because of the nearby r~17.6 magnitude guide star
TTGS
r~17.6mag
IRAS
K~11.6 mag, R~21
AO TTGS
Area
Gemini Observing
Tool View

30. The Future: SF Science with the JWST and ELT IFUs
FAINTER!
More Distant– Probe the Star formation process to low mass M stars, approaching the BD limit in the LMC and SMC!
Younger – Sun-Like stars at earlier epochs of formation – the “Class I” phase w/ envelope material remaining, or even younger!
Lower Mass – BDs and Free-Floating Planets in nearby star forming regions like Taurus and Orion!
Higher Mass – Massive O&B stars form in very dense cocoons of gas+dust, pierce through the extinction to see the forming stars!

31. Spectral Imaging of young Star Environments with JWST
The James Webb Space Telescope
The James Webb Space Telescope - operating at L2 in ~2014
6.5m Segmented Primary
4 Science Instruments:
NIRCam - Near-InfraRed Camera
NIRSpec - Near-InfraRed Spectrograph w/ IFU!
TFI - Tunable Filter Imager
MIRI - Mid-InfraRed Instrument w/ IFU
A schematic view of the JWST focal plane, including the placement of the science entrance apertures for each instrument.
NIRSpec and MIRI have Integral Field Units for very sensitive high-contrast spectral imaging of young star environments.

32. The Future: SF Science with IFUs on the ELTs
Nearby T Tauri stars are bright for large aperture telescopes – but we really need the ELT spatial resolution to push our observations to the ~Jupiter environs!
GMT
For Kinematics and spectral line detection/characterization, star formation science greatly benefits from HIGH spectral resolution! (R~20,000 or greater)
Mandell et al. (2009)
R~27,000
When considering properties for IFUs for large telescopes, please don’t forget about star formation science! & Consider a high spectral resolution IFU mode for the IR…!!
TMT

33. The Future: Next Generation Observations of T Tau?
Herbst et al. 1996
Data from Jan. 1995
Beck et al. 2008
Data from Oct. 2005
Next Generation
IFU View of T Tau
THANKS!! For Your Attention!